Hydrodynamical simulations of the decay of high-speed molecular turbulence. I. Dense molecular regions

Details Hydrodynamical simulations of the decay of high-speed molecular turbulence. I. Dense molecular regions Hydrodynamical simulations of the decay of high-speed molecular turbulence. I. Dense molecular regions

2002-08-15

arxiv.org/abs/astro-ph/0208293v1

Mon.Not.Roy.Astron.Soc. 337 (2002) 477

Astronomy and Astrophysics

Astrophysics

12 pages, 12 figures; For a version of the article with higher resolution figures, see http://star.arm.ac.uk/preprints/381.ps

Scientific paper

10.1046/j.1365-8711.2002.05927.x

We present the results from three dimensional hydrodynamical simulations of decaying high-speed turbulence in dense molecular clouds. We compare our results, which include a detailed cooling function, molecular hydrogen chemistry and a limited C and O chemistry, to those previously obtained for decaying isothermal turbulence. After an initial phase of shock formation, power-law decay regimes are uncovered, as in the isothermal case. We find that the turbulence decays faster than in the isothermal case because the average Mach number remains higher, due to the radiative cooling. The total thermal energy, initially raised by the introduction of turbulence, decays only a little slower than the kinetic energy. We discover that molecule reformation, as the fast turbulence decays, is several times faster than that predicted for a non-turbulent medium. This is caused by moderate speed shocks which sweep through a large fraction of the volume, compressing the gas and dust. Through reformation, the molecular density and molecular column appear as complex patterns of filaments, clumps and some diffuse structure. In contrast, the molecular fraction has a wider distribution of highly distorted clumps and copious diffuse structure, so that density and molecular density are almost identically distributed during the reformation phase. We conclude that molecules form in swept-up clumps but effectively mix throughout via subsequent expansions and compressions.

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